deletions | additions       diff --git a/The_Initial_Mass_Function_IMF__.tex b/The_Initial_Mass_Function_IMF__.tex  index eca2f8d..c066321 100644  --- a/The_Initial_Mass_Function_IMF__.tex  +++ b/The_Initial_Mass_Function_IMF__.tex 
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The Initial Mass Function (IMF) is a function that describes the distribution of mass of stars. Spiral galaxies are composed of all different types of stars ranging from massive stars, to low mass stars. The mass of a galaxy will always be constant as the galaxy ages, but the luminosity will change with age. This happens because as time progresses, stars run out of hydrogen in their core and turn off the Main Sequence. The most massive stars deplete their hydrogen supply quickest and are the first stars to leave the Main Sequence. Once the stars turn off the main sequence, they begin a fusion technique called shell burning. As the star ages, the luminosity changes because the stars radius increases and decreases. This happens the whole time the star is shell burning. Once that star has finished shell burning, it essentially stops contributing light to the galaxy. This means, that as galaxies age, the mass will always stay the same, but the luminosity will decrease with time because the massive some  stars have stopped contributing light to the galaxy.